Supernovae (SNe) are highly energetic phenomena injecting large amounts of energy (\(\sim \) e51 erg) and momentum, along with chemically enriched material into the interstellar medium (ISM) [1]}. They are considered to be a major source of interstellar turbulence and galactic outflows [2]}.
Their expanding leftovers, referred to as supernova remnants (SNRs), may interact with the ambient or even the parent molecular clouds (MCs) of their massive stellar precursors. This interaction compresses the gas and converts the kinetic energy to thermal energy; thus the gas is heated through the shock passage and the ram pressure of the parent MC is enhanced [3]}. All of this triggers chemical reactions which are otherwise unlikely or even impossible in MCs thereby boosting the abundance of molecular species that are usually rare in quiescent gas [4]}. One example of this is the detection of SiO emission from SNR W51C ([5]}), a well-established molecular tracer of shocks [6]}.
